J/MNRAS/440/1571 Herschel fluxes of Fornax galaxies (Fuller+, 2014) ================================================================================ The Herschel Fornax Cluster Survey II. FIR properties of optically selected Fornax cluster galaxies. Fuller C., Davies J.I., Auld R., Smith M.W.L., Baes M., Bianchi S., Bocchio M., Boselli A., Clemens M., Davis T.A., De Looze I., Di Serego Alighieri S., Grossi M., Hughes T.M., Viaene S., Serra P. =2014MNRAS.440.1571F ================================================================================ ADC_Keywords: Clusters, galaxy ; Galaxies, photometry ; Photometry, infrared ; Photometry, millimetric/submm Keywords: galaxies: clusters: individual: Fornax - galaxies: ISM - galaxies: photometry - infrared: galaxies Abstract: The Herschel Fornax Cluster Survey is a deep, far-infrared (FIR) survey of the Fornax cluster. The survey is in five Herschel bands (100-500{mu}m) and covers an area of 16deg^2^ centred on NGC 1399. This paper presents photometry, detection rates, dust masses, and temperatures using an optically selected sample from the Fornax Cluster Catalogue. Our results are compared with those previously obtained using data from the Herschel Virgo Cluster Survey (HeViCS). In Fornax, we detect 30 of the 237 (13%) optically selected galaxies in at least one Herschel band. The global detection rates are significantly lower than Virgo, reflecting the morphological make up of each cluster - Fornax has a lower fraction of late-type galaxies. For galaxies detected in at least three bands, we fitted a modified blackbody with a {beta}=2 emissivity. Detected early-type galaxies (E/S0) have a mean dust mass, temperature, and dust-to-stars ratio of log10(/M_{sun}_)=5.82+/-0.20, =20.82+/-1.77K, and log_10_(M_dust_/M_stars_)=-3.87+/-0.28, respectively. Late-type galaxies (Sa to Sd) have a mean dust mass, temperature, and dust-to-stars ratio of log10(M_dust_>/M_{sun}_)=6.54+/-0.19, =17.47+/-0.97K, and log_10_(M_dust_/M_stars_)=-2.93+/-0.09, respectively. The different cluster environments seem to have had little effect on the FIR properties of the galaxies and so we conclude that any environment-dependent evolution has taken place before the cluster was assembled. File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file tablea1.dat 254 237 Five band far-IR fluxes, uncertainties, and upper limits -------------------------------------------------------------------------------- See also: VII/180 : Galaxies in Fornax Cluster and five nearby groups (Ferguson+ 1990) Byte-by-byte Description of file: tablea1.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 3 I3 --- FCC [32/335] Fornax Cluster Catalog number (VII/180) 5- 6 I2 h RAh Right ascension (J2000) 8- 9 I2 min RAm Right ascension (J2000) 11- 15 F5.2 s RAs Right ascension (J2000) 17 A1 --- DE- Declination sign (J2000) 18- 19 I2 deg DEd Declination (J2000) 21- 22 I2 arcmin DEm Declination (J2000) 24- 27 F4.1 arcsec DEs Declination (J2000) 29 A1 --- l_S500 [<] Limit flag on S500 (1) 30- 50 F21.18 Jy S500 Herschel/SPIRE 500um flux or upper limit 52- 71 F20.18 Jy e_S500 ? rms uncertainty on S500 73 A1 --- l_S350 [<] Limit flag on S350 (1) 74- 94 F21.18 Jy S350 Herschel/SPIRE 350um flux or upper limit 96-116 F21.19 Jy e_S350 ? rms uncertainty on S350 118 A1 --- l_S250 [<] Limit flag on S250 (1) 119-140 F22.18 Jy S250 Herschel/SPIRE 250um flux or upper limit 142-161 F20.18 Jy e_S250 ? rms uncertainty on S250 163 A1 --- l_S160 [<] Limit flag on S160 (1) 164-186 F23.19 Jy S160 ?=- Herschel/PACS 160um flux or upper limit 188-208 F21.18 Jy e_S160 ?=- rms uncertainty on S160 210 A1 --- l_S100 [<] Limit flag on S100 (1) 211-232 F22.18 Jy S100 ?=- Herschel/PACS 1100um flux or upper limit 233-254 F22.19 Jy e_S100 ?=- rms uncertainty on S100 -------------------------------------------------------------------------------- Note (1): the upper limit is calculated from the 3{sigma} noise in the PSF convolved map. -------------------------------------------------------------------------------- History: From electronic version of the journal ================================================================================ (End) Patricia Vannier [CDS] 27-Jan-2015